Direct measurements from current and future missions will be able to provide time spectral series. In Fig.(REF ), right panel, we plot the simulated fluxes of two runs using POSSIS [1]} as a function of the EM rest wavelength. Run 1 (Run 2) corresponds to a \(q=1\)  BNS merger of \(1.4M_\odot \)  at 40 Mpc using the output of recent simulations[2]} \(M140140-LK\)  of DD2 (SHFo) EoS using polar/equatorial orientations. We notice that the early, agile KN follow up would be key to further constrain the EoS. The soft SFHo EoS peaks at IR, and is fainter than DD2 across the whole spectrum. Since the \(q\)  values remain the same we rely to the EoS features (including secondary peak features) for wavelengths less than \(\sim 1\mu \) m.
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